1995A&A...302..165G

It has been suggested that Fe I lines may constitute a major part of the many absorption lines observed in the (near-UV) solar spectrum and in those of late type stars. We use the table of Fe I lines recently measured in the laboratory by Nave et al. (1994) and examine the solar spectrum between 2756-2831A observed by us previously with the highest spectral resolution to date, R=1.75x10⁵. We exploit this existing observation since only such high spectral resolution allows sufficient isolation of weak lines in an underlying haze of absorption features. In this solar spectrum we detect ∼90% of the tabulated Fe I lines. Investigations of this kind are relevant, for instance, to primordial abundances of beryllium and boron in late type metal poor halo stars requiring complete model atmosphere line opacities and discrimination of possible line blending. We illustrate the case of Be with the spectrum of the late type star HD 165908 observed with R≃5x10⁴.